Properties of galaxy dark matter halos from weak lensing

a r X i v :a s t r o -p h /0306515v 2 13 J a n 2004

Draft version February 2,2008

Preprint typeset using L A T E X style emulateapj v.14/09/00

PROPERTIES OF GALAXY DARK MATTER HALOS FROM WEAK LENSING

Henk Hoekstra 1,2,3,H.K.C.Yee 2,3,and Michael D.Gladders 3,4

Draft version February 2,2008

ABSTRACT

We present the results of a study of weak lensing by galaxies based on 45.5deg 2of R C band imaging data from the Red-Sequence Cluster Survey (RCS).We de?ne a sample of lenses with 19.5

We present the ?rst weak lensing detection of the ?attening of galaxy dark matter halos.We use a simple model in which the ellipticity of the halo is f times the observed ellipticity of the lens.We ?nd

a best ?t value of f =0.77+0.18

?0.21,suggesting that the dark matter halos are somewhat rounder than the light distribution.The fact that we detect a signi?cant ?attening implies that the halos are well aligned with the light distribution.Given the average ellipticity of the lenses,this implies a halo ellipticity of

e halo =0.33+0.07

?0.09,in fair agreement with results from numerical simulations of CDM.We note that this result is formally a lower limit to the ?attening,since the measurements imply a larger ?attening if the halos are not aligned with the light distribution.Alternative theories of gravity (without dark matter)predict an isotropic lensing signal,which is excluded with 99.5%con?dence.Hence,our results provide strong support for the existence of dark matter.

We also study the average mass pro?le around the lenses,using a maximum likelihood analysis.We consider two models for the halo mass pro?le:a truncated isothermal sphere (TIS)and an NFW pro?le.We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo.The TIS model yields a best ?t velocity dispersion of σ=136±5±3km/s (all errors are 68%con?dence limits;the ?rst error bar indicates the statistical uncertainty,whereas

the second error bar indicates the systematic error)and a truncation radius s =185+30?28h

?1

kpc for a galaxy with a ?ducial luminosity of L B =1010h ?2

L B ⊙(under the assumption that the luminosity does not evolve with redshift).Alternatively,the best ?t NFW model yields a mass M 200=(8.4±0.7±

0.4)×1011h ?1M ⊙and a scale radius r s =16.2+3.6?2.9h

?1

kpc.This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.

Subject headings:cosmology:observations ?dark matter ?gravitational lensing ?galaxies:haloes

1.introduction

The existence of massive dark matter halos around galaxies is widely accepted,based on di?erent lines of ev-idence,such as ?at rotation curves of spiral galaxies (e.g.,Van Albada &Sancisi 1986)and strong lensing systems (e.g.,Keeton,Kochanek &Falco 1998).However,rela-tively little is known about the properties of dark matter halos.Strong lensing only probes the gravitational poten-tial on small (projected)scales,whereas the lack of visi-ble tracers at large radii hamper dynamical methods.To date,only satellite galaxies have provided some informa-tion (e.g.,Zaritsky &White 1994;McKay et al.2002;Prada et al.2003).

A promising approach to study the galaxy dark matter halos is weak gravitational lensing.The tidal gravitational ?eld of the dark matter halo introduces small coherent dis-tortions in the images of distant background galaxies.The weak lensing signal can be measured out to large projected distances from the lens,and hence provides a unique

1CITA,University of Toronto,Toronto,Ontario M5S 3H8,Canada 2

Department of Astronomy,University of Toronto,Toronto,Ontario M5S 3H8,Canada

3Visiting Astronomer,Canada-France-Hawaii Telescope,which is operated by the National Research Council of Canada,Le Centre National de Recherche Scienti?que,and the University of Hawaii 4Observatories of the Carnegie Institution of Washington,813Santa Barbara Street,Pasadena,California 91101

probe of the gravitational potential on large scales.

The applications of this approach are numerous:one can infer masses of galaxies and compare the results to their luminosities (e.g.,McKay et al.2001;Wilson et al.2001),or one can attempt to constrain the halo mass pro-?le (e.g.,Brainerd et al.1996;Hudson et al.1998;Fischer et al.2000;Hoekstra et al.2003).Also,weak lensing can be used to constrain the shapes of halos by measuring the azimuthal variation of the lensing signal.Unfortunately,one can only study ensemble averaged properties,because the weak lensing signal induced by an individual galaxy is too low to be detected.

A successful measurement of the lensing signal requires large samples of both lenses and background galaxies.The ?rst attempt to detect the lensing signal by galaxies was made by Tyson et al.(1984)using photographic plates.It took more than a decade and CCD cameras before the ?rst detections were reported (Brainerd et al.1996;Grif-?ths et al.1996;Dell’Antonio &Tyson 1996;Hudson et al.1998).These early results were limited by the small areas covered by the observations.

The accuracy with which the galaxy-galaxy lensing sig-nal can be measured depends on the area of sky that is observed,and on the availabitity of redshifts for the lenses (as it allows for a proper scaling of the lensing signal).Photometric redshifts were used by Hudson et al.(1998)to scale the lensing signal of galaxies in the Hubble Deep 1

2Properties of dark matter halos

Field,and by Wilson et al.(2001)who measured the lens-ing signal around early type galaxies as a function of red-shift.Furthermore,several lensing studies targeted regions covered by redshift surveys.Smith et al.(2001)used790 lenses from the Las Campanas Redshift Survey;Hoekstra et al.(2003)used1125lenses from the Canadian Net-work for Observational Cosmology Field Galaxy Redshift Survey(CNOC2).The areas covered by these surveys are relatively small.

The Sloan Digital Sky Survey(SDSS)combines both survey area and redshift information.Its usefulness for galaxy-galaxy lensing was demonstrated clearly by Fischer et al.(2000).More recently,McKay et al.(2001)used the available SDSS redshift information to study the galaxy-galaxy lensing signal as a function of galaxy properties (also see Guzik&Seljak2002;Seljak2002).

The data used in this paper currently lacks redshift in-formation for the lenses.However,compared to previous work,the combination of large area and depth of our obser-vations allow us to measure the galaxy lensing signal with great precision.We use45.5deg2of R C-band imaging data from the Red-Sequence Cluster Survey(RCS).These data have been used previously for several weak lensing studies.Hoekstra et al.(2002a;2002b)placed joint con-straints on?m andσ8by measuring the lensing signal caused by large scale structure.Related to the subject of this paper is the study of the bias parameters as a func-tion of scale by Hoekstra et al.(2001b)and Hoekstra et al. (2002c).The latter studies made use of the galaxy-mass cross-correlation function measured from the RCS data. Here we use the galaxy-mass cross-correlation function for a di?erent purpose:we e?ectively deconvolve the cross-correlation function to study the properties of dark matter halos surrounding galaxies at intermediate redshifts.

The structure of the paper is as follows.In§2we brie?y discuss the data and the redshift distributions of the lenses and the sources.The ensemble averaged tangential shear around the lenses(galaxy-mass cross-correlation function) is presented in§3.In§4we use a maximum likelihood analysis to derive constraints on the extent of dark matter halos.The measurement of the projected shapes of the halos is presented in§5.

2.observations and analysis

We use the R C-band imaging data from the Red-Sequence Cluster Survey(Yee&Gladders2001;Gladders &Yee2003).The complete survey covers90deg2in both R C and z′,spread over22widely separated patches of ～2.1×2.3degrees.In this paper we use data from the northern half of the survey,which consists of10patches, observed with the CFH12k camera on the CFHT.These data cover45.5deg2on the sky,but because of masking the e?ective area is somewhat smaller.In the lensing anal-ysis we use a total of42deg2.A detailed description of the data reduction and object analysis can be found in Hoek-stra et al.(2002a),to which we refer for technical details. Here we present a short description of the various steps in the analysis.

We use single exposures in our analysis,and conse-quently cosmic rays have not been removed.However, cosmic rays are readily eliminated from the photometric catalogs:small,but very signi?cant objects are likely to be cosmic rays,or artifacts from the CCD.The object ?nder gives fair estimates of the object sizes,and we re-move all objects smaller than the size of the PSF.Some faint cosmic rays may hit galaxies,and consequently might not be recognized as cosmic rays.Based on the number of cosmic ray hits,and the area covered by galaxies we?nd that less than0.2%of the galaxies might be a?ected.Also, cosmic rays only introduce additional noise in the shape measurement,but do not bias the result.Consequently we conclude that remaining cosmic rays have a negligble e?ect on our results.

The objects in this cleaned catalog are then analysed, which yield estimates for the size,apparent magnitude, and shape parameters(polarisation and polarisabilities). The objects in this catalog are inspected by eye,in order to remove spurious detections.These objects have to be removed because their shape measurements are a?ected by cosmetic defects(such as dead columns,bleeding stars, halos,di?raction spikes)or because the objects are likely to be part of a resolved galaxy(e.g.,HII regions).

To measure the small,lensing induced distortions in the images of the faint galaxies it is important to accurately correct the shapes for observational e?ects,such as PSF anisotropy,seeing and camera shear;PSF anisotropy can mimic a cosmic shear signal,and a correction for the see-ing is required to relate the measured shapes to the real lensing signal.To do so,we follow the procedure outlined in Hoekstra et al.(1998).We select a sample of mod-erately bright stars from our observations,and use these to characterize the PSF anisotropy and seeing.We?t a second order polynomial to the shape parameters of the selected stars for each chip of the CFH12k camera.These results are used to correct the shapes of the galaxies for PSF anisotropy and seeing.

The e?ect of the PSF is not the only observational dis-tortion that has to be corrected.The optics of the camera stretches the images of galaxies(i.e.,it introduces a shear) because of the non-linear remapping of the sky onto the CCD.We have used observations of astrometric?elds to ?nd the mapping between the sky and the CCD pixel co-ordinate system,and derived the corresponding camera shear,which is subsequently subtracted from the galaxy ellipticity(see Hoekstra et al.1998).

The?ndings presented in Hoekstra et al.(2002a)sug-gest that the correction for PSF anisotropy has worked well.The absence of a“B”-mode on large scales in the measurements of the cosmic shear(Hoekstra et al.2002b) provides additional evidence that systematics are well un-der control(the small scale“B”-mode is attributed to intrinsic alignments).Furthermore,cosmic shear studies are much more sensitive to systematics than galaxy-galaxy lensing measurements(e.g.,see Hoekstra et al.2003).In galaxy-galaxy lensing one measures the lensing signal that is perpendicular to the lines connecting many lens-source pairs.These connecting lines are randomly oriented with respect to the PSF anisotropy,and hence suppress any residual systematics.

2.1.Redshift distributions

For the analysis presented here,we select a sample of “lenses”and“sources”on the basis of their apparent R C magnitude.We de?ne galaxies with19.5

Hoekstra et al.3

as lenses,and galaxies with21.5

For a singular isothermal sphere,the amplitude of the lensing signal depends on β ,the average ratio of the an-gular diameter distances between the lens and the source, D ls,and the distance between the observer and the source D s.More general,the signal also depends on D l,the dis-tance between the observer and the lens.Hence,to inter-pret the measurements,such as size and mass,one needs to know the redshift distributions of both lenses and sources. The CNOC2Field Galaxy Redshift Survey(e.g.,Lin et al.1999;Yee et al.2000;Carlberg et al.2001) has measured the redshift distribution of?eld galaxies down to R C=21.5,which is ideal,given our limits of 19.5

Compared to studies using SDSS data(McKay et al. 2001)we have the disadvantage that we do not have(spec-troscopic)redshifts for the individual lenses.As shown by Schneider&Rix(1997)and Hoekstra et al.(2003) this limits the accuracy of the measurements.We can de-rive useful constraints on the masses and extent of dark matter halos,but we have to assume scaling relations be-tween these parameters and the luminosity of the galaxies. Multi-color data for the northern part of the RCS will be available in the near future,allowing us to select a sample of lenses based on their photometric redshifts,and con-strain the scaling relations.

Nevertheless,the large area covered by the RCS allows us to derive interesting information about the properties of the lenses.In§4we use di?erent cuts in apparent mag-nitude to study the properties of dark matter halos using a maximum likelihood analysis.

For the source galaxies the situation is more compli-cated.These galaxies are generally too faint for spec-troscopic surveys,although recently Cohen et al.(2000) measured spectroscopic redshifts around the Hubble Deep Field North down to R C～24.Cohen et al.(2000)?nd that the spectroscopic redshifts agree well with the photometric redshifts derived from multi-color photome-try.Because of likely?eld-to-?eld variations in the red-shift distribution,we prefer to use the photometric red-shift distributions derived from both Hubble Deep Fields (Fern′a ndez-Soto et al.1999),which yields a median red-shift of z=0.53for the source galaxies.

The adopted source and lens redshift distributions result in an average value of β =0.29±0.01(average for the full sample of lenses and sources),where the error bar is based on the?eld-to-?eld variation and the?nite number of galaxies in the Hubble Deep Fields.The uncertainty in β a?ects predominantly our estimates for the galaxy masses(and velocity dispersions),but is negligible for the other model parameters.We note that for the galaxy-galaxy lensing analysis presented here the relevant param-eter is L0.3Bβ ,as opposed to simply β ,but we have veri?ed that results in a negligible change in the adopted systematic error.Throughout the paper we indicate the systematic error in the masses and velocity dispersions by a second error

bar.

Fig.1.—(a)The galaxy-mass cross-correlation function as a func-tion of angular scale.The lenses are selected on the basis on their apparent R C-band magnitude,taking19.5

3.galaxy-mass cross-correlation function The galaxy-mass cross-correlation function provides a convenient way to present the measurements.It is ob-tained from the data by measuring the tangential align-ment of the source galaxies with respect to the lens as a function of radius.Its use for studying the halos of galaxies is limited,because the clustering of galaxies complicates a direct interpretation of the signal:on small scales the signal is dominated by the mass distribution of the lens, but on larger scales one measures the superposition of the contributions from many lenses.

The observed galaxy-mass cross-correlation function as a function of angular scale is presented in Figure1a.A sig-ni?cant signal is detected out to one degree from the lens. If the signal presented in Figure1a is caused by gravita-tional lensing,no signal should be present when the phase of the distortion is increased byπ/4(i.e.,when the sources are rotated by45degrees).The results of this test,shown in Figure1b,suggest that residual systematics are negli-gible.

Before we can interpret the results we need to exam-ine the contribution of foreground galaxies.Some of the source galaxies will be in front of the lenses,and lower the lensing signal independent of radius.This is absorbed in

4Properties of dark matter halos

the value of β .These galaxies decrease the lensing sig-nal independent of angular scale.Some sources,however,are physically associated with the lenses.These galaxies cluster around the lenses,a?ecting the lensing signal more on small scales.We need to account for this source of contamination.To do so,we measure a fractional excess of sources around lenses which decreases with radius as f bg (r )=0.93r ?0.76(r in arcseconds),similar to what was found by Fischer et al.(2000).Under the assumption that the orientations of these galaxies are random (the tidal in-teraction with the lens has not introduced an additional tangential or radial alignment),the observed lensing signal has to be increased by a factor 1+f bg (r ).This assump-tion is supported by the ?ndings of Bernstein &Norberg (2002)who examined the tangential alignment of satellite galaxies around galaxies,extracted from the 2dF Galaxy Redshift Survey.The measurements presented in Figures 1have been corrected for this decrease in signal.We note that the correction for the presence of satellite galaxies is small,and has no signi?cant e?ect on our

results.

Fig. 2.—(a)Ensemble averaged tangential shear as a function of radius out to 2arcminutes from the lens.The solid line corre-sponds to the best ?t SIS model to the data at radii smaller than 2arcminutes.(b)The signal when the phase of the shear is increased by π/4.Note the di?erent vertical scale between panels a and b.

The signal on small angular scales is dominated by a single lens galaxy,and can be used to obtain an estimate of the mass weighted velocity dispersion of the sample of lenses (although such a mass estimate can still be slightly biased because of the clustering of the lenses).Figure 2a shows the ensemble averaged tangential shear on small scales.The measurements presented in Figure 2b show no evidence for residual systematics.

We ?t a singular isothermal sphere (SIS)model to the tangential shear at radii smaller than 2arcminutes (which corresponds to ～350h ?1kpc at the mean redshift of the lenses).The best ?t model is indicated by the dashed line in Figure 2a.For the Einstein radius r E we obtain a value of r E =0.′′140±0.′′009.If we extend the ?t to much larger

radii,the inferred value for the Einstein radius increases systematically.With our adopted redshift distributions for the lenses and the sources,the value of r E corresponds to a value of σ2 1/2=128±4km/s.The corresponding circular velocity can be obtained using V c =

√

Hoekstra et al.5 tributed in common halos,a simple interpretation of the

results becomes more di?cult.

Hoekstra et al.(2003)examined how known groups in

their observed?elds a?ected the lensing results,and found

that the masses and sizes might be overestimated by at

most～10%.Guzik&Seljak(2002)found similar results

from their analysis of the galaxy-galaxy lensing signal in

the context of halo models.Their approach allows one to

separate the contribution from groups to the lensing signal.

As expected,Guzik&Seljak(2002)found that the e?ect

depends on galaxy type:early type galaxies are found in

high density regions,and are a?ected more.Alternatively,

a comparison with numerical simulations which include a

prescription for galaxy formation(e.g.,Kau?mann et al.

1999a,1999b;Guzik&Seljak2001)can be used to quan-

tify this e?ect.

Another complication is the fact that we cannot sep-

arate the lenses in di?erent morphology classes with the

current data.Early and late type galaxies of a given lu-

minosity have di?erent masses,etc.(e.g.,Guzik&Seljak

2002).Hence,it is important to keep in mind that the re-

sults presented here are ensemble averages over all galaxy

types.This is where the SDSS can play an important role,

although we can signi?cantly improve the RCS results with

upcoming multi-color data.

The variance in the polarisations is approximately con-

stant with apparent magnitude and we approximate the

distribution by a Gaussian distribution.With the lat-

ter assumption,the log-likelihood follows aχ2distribution

with the number of degrees of freedom equal to the num-

ber of free model parameters,and the determination of

con?dence intervals is straightforward.The log-likelihood

is given by the sum over the two components of the polar-

isation e i of all the source galaxies

log L=? i,j e i,j?Pγj g model i,j2πGr2(r2+s2),(2)

whereσis the line-of-sight velocity dispersion,and s is a

truncation scale,i.e.the radius where the pro?le steepens.

On small scales(r?s)the model behaves as an Singular

Isothermal Sphere(SIS)model,whereas for r?s the den-

sity decreases∝r?4.The mass contained within a sphere

of radius r is given by

M(r)=

2σ2s

G

s=7.3×1012 σ1Mpc .(4)

The projected surface density for this model is given by

Σ(r)=σ2

√

6Properties of dark matter halos

relations,which allow us to relate the halo properties of the lenses to those of a ?ducial galaxy.For the ?ducial galaxy we take a luminosity of L B =1010h ?2L B ⊙.

Dynamical studies provide evidencence of a power law scaling relation between the velocity dispersion and the lu-minosity (e.g.,Tully-Fisher relation for spiral galaxies and Faber-Jackson relation for early type galaxies).We assume

σ∝L 0.3

B ,which is based on the observed slope of the B -band Tully-Fisher relation (e.g.,Verheijen 2001).Little is known,however,about the relation of the extent of dark matter halos with other (observable)https://www.doczj.com/doc/c317610808.html,ing

SDSS data,Guzik &Seljak (2002)?nd that M ∝L 1.2±0.2

g ′

.Motivated by this result,we adopt s ∝L 0.6

B ,which gives a total mass M ∝L 1.2B .We note,however,that we probe lower luminosities than Guzik &Seljak (2002)(also see McKay et al.2001)and as a result,the adopted scaling relation might di?er from the actual

ones.

Fig.3.—Joint constraints on the velocity dispersion σand trunca-tion parameter s for a ?ducial galaxy with L B =1010h ?2L B ⊙.The contours indicate the 68.3%,95.4%,and the 99.7%con?dence on two parameters jointly.The cross indicates the best ?t value.The dashed lines indicate models with masses M tot =10×1012h ?1M ⊙and M 200=5×1012h ?1M ⊙.

Figure 3shows the joint constraints on the velocity dis-persion σand truncation parameter s for a ?ducial galaxy

with L B =1010h ?2L B ⊙,under the assumption that the luminosity does not evolve with redshift.Conveniently,for this particular luminosity,the inferred values of the velocity dispersion and truncation parameter depend only marginally on the adopted scaling relations.

For the velocity dispersion we obtain a value of σ=136±5±3km/s (68%con?dence,marginalizing over all other model paremeters).Hoekstra et al.(2003)?nd a velocity dispersion of σ=110±12for a galaxy with a luminosity of 5.6×109h ?2L B ⊙.For a galaxy with that luminosity,the adopted scaling relations imply a velocity dispersion of 114±4±2km/s,in excellent agreement with Hoekstra et al.(2003).McKay et al.(2001)who found a best ?t value of σ=113+17?13km/s (95%con?dence)for

a galaxy with L g ′～9×109h ?2L g ′⊙.Our results corre-spond to a velocity dispersion of σ=127±5±3km/s for a galaxy of that luminosity,in good agreement with the SDSS result.

We derive tight constraints on the truncation param-eter,i.e.the extent of dark matter halos.We ?nd a

value of s =185+30?28h

?1

kpc (68%con?dence),and a to-tal mass M tot =(2.5±0.3±0.1)×1012h ?1M ⊙.The results presented in Hoekstra et al.(2003)imply a value

of s =290+139?82h

?1

kpc (68%con?dence)for their ?ducial galaxy.For a galaxy with a luminosity of 5.6×109h ?2L B ⊙,

we obtain s =131+21?20h ?1

kpc,marginally consistent with Hoekstra et al.(2003).

If we assume that L B ∝(1+z )we obtain a velocity dispersion of σ=146±5±3km/s and a truncation size

of s =213+35?32h

?1

kpc for a galaxy with L B (z =0)=1010h ?2

L B ⊙.

4.2.NFW model

Numerical simulations of collisionless cold dark matter (CDM)reproduce the observed structure in the universe remarkably well.Furthermore these simulations suggest that CDM gives rise to a speci?c density pro?le,which ?ts the radial mass distribution for halos with a wide range in mass (e.g.,Dubinski &Carlberg 1991;Navarro et al.1995,1996,1997).The NFW density pro?le is characterized by 2parameters,a density contrast δc and a scale r s

ρ(r )=

δc ρc

3

ρc r 3200,

(7)

with a corresponding rotation velocity V 200of

V 200=V (r 200)=

GM 200

3

c 3

Hoekstra et al.

7

test of the assumption that structures form through dissi-pationless collapse.The predicted pro?les agree well with the observed mass distribution in clusters of galaxies (e.g.,Hoekstra et al.2002d),but the situation is less clear for galaxy mass halos.Rotation curves can provide some con-straints,but typical values for r s for galaxy mass halos are 10?20h ?1kpc,comparable to the outermost point for which rotation curves have been measured.

Galaxies that are thought to be dark matter dominated,such as low surface brightness galaxies,potentially might be more suitable to test the CDM predictions.Studies of the rotation curves of low surface brightness galaxies suggest that,at least for a fraction of them,the observed rotation curves rise more slowly than the CDM predictions (e.g,de Blok,McGaugh &Rubin 2001;McGaugh,Barker &de Blok 2002).It is not clear,however,whether such studies provide a good test of CDM,because low surface brightness galaxies are peculiar (Zwaan &Briggs 2000),and their formation is not well understood.Hence,it is not obvious that their halos should be described by an NFW pro?le.Recently Ricotti (2003)has suggested that the inner slope might depend on halo mass,with low mass systems having shallow cores,whereas massive galaxies are well described by the NFW pro?le.

In this section we compare the NFW pro?le to the obser-vations,with δc and r s as free parameters.The equations describing the shear for the NFW pro?le have been derived by Bartelmann (1996)and Wright &Brainerd (2000).As before we have to adopt scaling relations.We as-sume that the maximum rotation velocity scales ∝L 0.3

B (the B-band Tully-Fisher relation;Verheijen 2001).If we

also assume that M 200∝L 1.2

B ,as motivated by the ?nd-ings of Guzik &Seljak (2002),we obtain that r s ∝L 0.75B

and δc ∝L ?0.85

B

.Figure 4shows the joint constraints on V 200and r s for a galaxy with a luminosity of L B =1010h ?2L B ⊙.In addi-tion,the right axis indicates the corresponding values for M 200.We derive a best ?t value of V 200=162±5±3km/s,or M 200=(8.4±0.7±0.4)×1011h ?1M ⊙(68%con?dence),

and a corresponding value of r 200=139+3?5h

?1

kpc.It is useful to compare this result with the mass from the TIS model.

The TIS model yields M TIS (r 200)=(1.0±0.1)×1012h ?1M ⊙,which is slightly larger than the NFW value.As shown by Wright &Brainerd (2000),isothermal mod-els give higher masses compared to NFW models.Hence,the results derived from both models are consistent.

From their galaxy-galaxy lensing analysis of the SDSS,Guzik &Seljak (2002)?nd M 200=(9.3±1.6)×1011h ?1M ⊙for a galaxy of L g ′～1.1×1010h ?2L g ′⊙,in good agreement with our results.

For the scale r s we ?nd r s =16.2+3.6?2.9h

?1

kpc (68%con?dence),and the best ?t density contrast is δc =

2.4+1.4?0.8×104

(68%con?dence;con?dence interval from Monte Carlo simulation).The TIS model provides a slightly better ?t to the data,but the di?erence is not signi?cant,and consequently the data are not su?cient to distinguish between the NFW and TIS model.

As before,we also calculated the results under the as-sumption that the luminosity evolves ∝(1+z ).In this

case we ?nd a value of r s =17.2+3.8?3.1h

?1

kpc and V 200=176±5±4km/s for a L B (z =0)=1010h ?2L B ⊙galaxy.

In our maximum likelihood analysis we considered r s and V 200(or equivalently the mass M 200)as free parame-ters.Numerical simulations of CDM,however,show that the parameters in the NFW model are correlated,albeit with some scatter.As a result,the NFW model can be considered as a one-parameter model:given the cosmol-ogy,redshift,and one of the NFW parameters,the values for all other parameters can be computed using the rou-tine CHARDEN made available by Julio Navarro 1.Hence,the simulations make a de?nite prediction for the value of V 200as a function of r s .The dotted line in Figure 4in-dicates this prediction.If the simulations provide a good description of dark matter halos,the dotted line should intersect our con?dence region,which it does.

This result provides important support for the CDM paradigm,as it predicts the correct “size”of dark matter halos.It is important to note that this analysis is a di-rect test of CDM (albeit not conclusive),because the weak lensing results are inferred from the gravitational poten-tial at large distances from the galaxy center,where dark matter dominates.Most other attempts to test CDM are con?ned to the inner regions,where baryons are,or might be,

important.

Fig.4.—Joint constraints on δc r 2s and scale radius r s

for a ?du-cial galaxy with L B =1010h ?2L B ⊙,with an NFW pro?le.The

contours indicate the 68.3%,95.4%,and the 99.7%con?dence on two parameters jointly.The cross indicates the best ?t value.The dashed lines indicate models with masses M 200=5×1011h ?1M ⊙and M 200=1012h ?1M ⊙.The dotted line indicates the predictions from the numerical simulations,which are in excellent agreement with our results.

5.shapes of halos

The average shape of dark matter halos can provide important information about the nature of dark matter.Numerical simulations of cold dark matter yield triaxial halos,with a typical ellipticity of ～0.3(e.g.,Dubinski &

1

The routine CHARDEN can be obtained from http://pinot.phys.uvic.ca/?jfn/charden

8Properties of dark matter halos

Carlberg1991).Hence,in the context of collisionless cold dark matter,the theoretical evidence for?attened halos is quite strong.If the dark matter is interacting,it tends to produce halos that are more spherical(compared to cold dark matter).This di?erence is more pronounced in the central parts of the halo,where the density is high.On the large scales probed by weak lensing,the di?erent types of dark matter(for reasonable interaction cross-sections) produces halos with similar shapes.

Nevertheless,a measurement of the average shape of dark matter halos is important,because the observational evidence is still limited.Dynamical measurements are limited by the lack of visible tracers,and therefore only probe the vertical potential on scales≤15kpc.Although the spread in inferred values for the axis ratio c/a(where c/a is the ratio of the shortest to longest principle axis of the halo)is large,the results suggest an average value of c/a=0.5±0.2(Sackett1999).

Weak gravitational lensing is potentially the most pow-erful way to derive constraints on the shapes of dark mat-ter halos.The amount of data required for such a mea-surement,however,is large(e.g.,Brainerd&Wright2000; Natarajan&Refregier2000):the galaxy-galaxy lensing signal is small,and now one needs to measure an even smaller azimuthal variation.We also have to assume that the galaxy and its halo are aligned.An imperfect align-ment between light and halo will reduce the amplitude of the azimuthal variation detectable in the weak lensing analysis.Hence,weak lensing formally provides a lower limit to the average halo ellipticity.

Brainerd&Wright(2000)and Natarajan&Refregier (2000)proposed to study the azimuthal variation in the tangential shear around the lenses.On very small scales, the lensing signal is dominated by the lens,but on larger scales,the clustering of the lenses will lower the signal one tries to measure(the two point function is axisymmetric). We therefore use the maximum likelihood approach used in the previous section.

To maximize the signal-to-noise ratio of the measure-ment one has to assign proper weights to the lenses:edge-on galaxies have maximal weight,whereas the lensing sig-nal around face-on galaxies contains no information about the shape of the halo.We adopt a simple approach, and assume that the(projected)ellipticity of the dark matter halo is proportional to the shape of the galaxy: e halo=fe lens.

The measurement of the azimuthally averaged tangen-tial shear around galaxies is robust against residual sys-tematics(e.g.,imperfect correction for PSF anisotropy): contributions from a constant or gradiant residual shear cancel.This is no longer the case for the quadrupole sig-nal,and imperfect correction for the PSF anisotropy can mimick the signal from a?attened halo.

If the lens galaxy is oriented randomly with respect to the residual shear,the average over many lenses will can-cel the contribution from systematics.In real data,how-ever,the uncorrected shapes of the lenses are aligned with the systematic signal.Hence,an imperfect correction can give rise to a small quadrupole signal,although we note that the lenses used in our analysis are large compared to the PSF.We estimate the amplitude of this e?ect in Ap-pendix A,and show that it is negligible for the measure-ments presented here.We also examined the robustness of our results by splitting the data into two samples and comparing the

results.

Fig.5.—?χ2as a function of f.We have assumed that the ellip-ticity of the halos is related to the observed ellipticity of the lens as e halo=fe lens.We have indicated the68.3%and95.4%con?dence

intervals.We?nd a best?t value of f=0.77+0.18

?0.21

(68%con?dence). Round halos(f=0)are excluded with99.5%con?dence.

We use an elliptical TIS model to compute the model shear?eld,and compare this to the data.Figure5shows the resulting?χ2as a function of f.We?nd a best?t

value of f=0.77+0.18

?0.21

(68%con?dence).This suggests that,on average,the dark matter distribution is rounder than the light distribution.As discussed above,our analy-sis formally provides only a lower limit on the halo elliptic-ity,and the true ellipticity might be higher if some of the halos are misaligned with the light.Nevertheless,the fact that we detect a signi?cant?attening implies that the ha-los are well aligned with the light distribution.Also note that the lensing signal is caused by a range of di?erent galaxy types,for which our simple relation between the halo ellipticity and light distribution might not be valid. Consequently the interpretation of the results is di?-cult,although a simple interpretation actually yields sen-sible results.For instance,the average ellipticity of the lens galaxies is e lens =0.414.Hence,the measured value of f implies an average projected halo ellipticity of

e halo =0.33+0.07

?0.09

(68%con?dence),which corresponds

to an projected axis ratio of c/a=0.67+0.09

?0.07

(68%con?-dence;where we have used c/a=1?e).Although the weak lensing yields a projected axis ratio,the result is in fair agreement with the results from numerical simulations.

A robust outcome of our analysis is that spherical ha-los(f=0)are excluded with99.5%con?dence.As we demonstrate below,this poses serious problems for alter-native theories of gravity,which attempt to explain the observations without dark matter.

Hoekstra et al.

9

5.1.Implications for alternative theories of gravity In this section we examine the implications of our mea-surement of the anisotropy in the lensing signal around galaxies for theories of gravity without dark matter.We focus on one particular approach:Modi?ed Newtonian Dynamics (MOND;Milgrom 1983;Sanders 1986;Sanders &McGaugh 2002),which has been shown to describe rota-tion curves rather well (e.g.,Begeman et al.1991;Sanders &Verheijen 1998).

In principle weak lensing can be used as a powerful test of MOND,but unfortunately no relativistic description of MOND has been found.Consequently one cannot com-pute the lensing signal in this theory.However,even in the absence of an appropriate description of lensing,we can use the observed anisotropy in the lensing signal around galaxies to test MOND.

In any reasonable alternative theory of gravity,the anisotropy in the lensing signal of an isolated galaxy is caused by the distribution of light and gas in that galaxy.In order to explain the ?at rotation curves,these alterna-tive theories typically need an e?ective force law ∝r ?1.Hence,on small scales one expects an anisotropic signal,but at large radii (where there are no stars and gas)we assume that the anisotropy in the lensing signal decreases ∝r ?2.As a result,these theories predict an almost isotropic weak lensing signal on the scales probed by our analysis,which is not observed.

Galaxies,however,are not isolated and the external ?eld e?ect (Milgrom 1986)might complicate the interpretation of our measurements.In MOND,if a galaxy is embed-ded in an external ?eld,this ?eld dominates the dynamics if its acceleration is larger than the acceleration of the galaxy.As a result,the e?ective gravitational ?eld is non-spherical,even if the potential of the galaxy is isotropic (as is the case for an isolated galaxy).

This e?ect is important if galaxies would be aligned with this external ?eld.We know,however,that the intrinsic alignments of galaxies are small (e.g.,Lee &Pen 2001,2002)and for the measurements presented here,it is safe to assume that the lenses have random orientation with respect to any external ?eld.Consequently,the observed anisotropy in the lensing signal cannot be caused by the external ?eld e?ect.

Hence,our ?ndings provide strong support for the exis-tence of dark matter,because alternative theories of grav-

ity predict an almost isotropic lensing signal.Better con-straints can be derived from future weak lensing surveys,which will allow us to study the anisotropy a function of projected distance from the galaxy.

6.conclusions

We have analysed the weak lensing signal caused by a sample of lenses with 19.5

The TIS model yields a best ?t velocity dispersion of σ=136±5±4km/s and a truncation radius s =

185+30?28h

?1

kpc for a galaxy with a ?ducial luminosity of L B =1010h ?2L B ⊙.Alternatively,the best ?t NFW model yields a mass M 200=(8.4±0.7±4)×1011h ?1M ⊙

and a scale radius r s =16.2+3.6?2.9h

?1

kpc.This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.

We also present the ?rst detection of the ?attening of galaxy dark matter halos from weak lensing.We use a sim-ple model in which the ellipticity of the halo is f times the observed ellipticity of the lens.We ?nd a best ?t value

of f =0.77+0.18

?0.21(68%con?dence),suggesting that the dark matter halos are somewhat rounder than the light distribution.The fact that we detect a signi?cant ?at-tening implies that the halos are aligned with the light distribution.Given the average ellipticity of the lenses,

this implies a halo ellipticity of e halo =0.33+0.07

?0.09(68%con?dence),in fair agreement with results from numerical simulations of CDM.This result provides strong support for the existence of dark matter,as an isotropic lensing signal is excluded with 99.5%con?dence.

We are grateful to the anonymous referee whose com-ments have signi?cantly improved the quality of this pa-per.The RCS project is partially supported by grants from the Natural Science and Engineering Science Coun-cil of Canada and the University of Toronto to HKCY.

APPENDIX

contribution of systematics to the shape measurement of dark halos

In this appendix we examine how residual systematics a?ect the measurement of the ?attening of dark matter halos.A schematic overview of the situation is presented in Figure A6.The thin lines indicate the direction of residual systematics.The residual shear has an amplitude ?γand a position angle φwith respect to the major axis of the lens.The tangential

shear γobs T observed at a position (r,θ)is the sum of the lensing signal γlens

T and the contribution from systematics ?γT .The latter is given by

?γT =??γ[cos(2φ)cos(2θ)+sin(2φ)sin(2θ)]=??γcos(2(θ?φ)).(A1)

Hence,the azimuthally averaged tangential shear is not a?ected by systematics as

dθ?γT (θ)=0,and the weak lensing

mass estimate is very robust.For a ?attened halo,the lensing signal γlens

T is given by

γlens

T (r,θ)=[1+γf cos(2θ)]· γT (r ),

(A2)

10Properties of dark matter halos

where γT is the azimuthally averaged tangential shear,andγf is a measure of the?attening of the halo.For positive values ofγf,the halo is aligned with the lens.

We consider the worst case scenario,and demonstrate that even in this situation the results are robust.One way to estimate the?attening of the halo is to measure the shearsγ+(atθ=0andπ),andγ?(atθ=π/2and3π/2).The observed ratio f=γ?/γ+is

γ?+?γcos(2φ)

f obs=

γ21+γ22,we?nd

cos(2φ) =α?γ

π

.(A5)

2σ

This introduces a relatively large signal because face-on lenses(γ≈0)align easily with the PSF anisotropy.Such lenses,however,contain no information about the shape of the halo.In our analysis we assign a weight∝γto each lens. Hence in our case we are less sensitive to systematics as the correct estimate is given by

cos(2φ) =α?γ

Hoekstra et al.11 Hence,the observed ratioγ?/γ+reduces to

γ?+?γ2α/2

f obs=

门禁系统使用说明书

安装、使用产品前，请阅读安装使用说明书。 请妥善保管好本手册，以便日后能随时查阅。 GST-DJ6000系列可视对讲系统 液晶室外主机 安装使用说明书 目录 一、概述 (1) 二、特点 (2) 三、技术特性 (3) 四、结构特征与工作原理 (3) 五、安装与调试 (5) 六、使用及操作 (10) 七、故障分析与排除 (16) 海湾安全技术有限公司

一概述 GST-DJ6000可视对讲系统是海湾公司开发的集对讲、监视、锁控、呼救、报警等功能于一体的新一代可视对讲产品。产品造型美观，系统配置灵活，是一套技术先进、功能齐全的可视对讲系统。 GST-DJ6100系列液晶室外主机是一置于单元门口的可视对讲设备。本系列产品具有呼叫住户、呼叫管理中心、密码开单元门、刷卡开门和刷卡巡更等功能，并支持胁迫报警。当同一单元具有多个入口时，使用室外主机可以实现多出入口可视对讲模式。 GST-DJ6100系列液晶室外主机分两类（以下简称室外主机），十二种型号产品： 1.1黑白可视室外主机 a)GST-DJ6116可视室外主机（黑白）； b)GST-DJ6118可视室外主机（黑白）； c)GST-DJ6116I IC卡可视室外主机（黑白）； d)GST-DJ6118I IC卡可视室外主机（黑白）； e)GST-DJ6116I（MIFARE）IC卡可视室外主机（黑白）； f)GST-DJ6118I（MIFARE）IC卡可视室外主机（黑白）。 1.2彩色可视液晶室外主机 g)GST-DJ6116C可视室外主机（彩色）； h)GST-DJ6118C可视室外主机（彩色）； i)GST-DJ6116CI IC卡可视室外主机（彩色）； j)GST-DJ6118CI IC卡可视室外主机（彩色）； k)GST-DJ6116CI（MIFARE）IC卡可视室外主机（彩色）； GST-DJ6118CI（MIFARE）IC卡可视室外主机（彩色）。 二特点 2.1 4*4数码式按键，可以实现在1~8999间根据需求选择任意合适的数字来 对室内分机进行地址编码。 2.2每个室外主机通过层间分配器可以挂接最多2500台室内分机。 2.3支持两种密码（住户密码、公用密码）开锁，便于用户使用和管理。 2．4每户可以设置一个住户开门密码。 2.5采用128×64大屏幕液晶屏显示，可显示汉字操作提示。 2.6支持胁迫报警，住户在开门时输入胁迫密码可以产生胁迫报警。 2.7具有防拆报警功能。 2.8支持单元多门系统，每个单元可支持1～9个室外主机。 2.9密码保护功能。当使用者使用密码开门，三次尝试不对时，呼叫管理中 心。 2.10在线设置室外主机和室内分机地址，方便工程调试。 2.11室外主机内置红外线摄像头及红外补光装置，对外界光照要求低。彩色 室外主机需增加可见光照明才能得到好的夜间补偿。 2.12带IC卡室外主机支持住户卡、巡更卡、管理员卡的分类管理，可执行 刷卡开门或刷卡巡更的操作，最多可以管理900张卡片。卡片可以在本机进行注册或删除，也可以通过上位计算机进行主责或删除。

电动汽车拆解分析报告

电动汽车拆解分析报告 精品汇编资料 【电动汽车拆解】PCU（一）：采用双面冷却构造实现小型化 电装已开始向丰田汽车的部分混合动力车型提供PCU（功率控制单元）。丰田汽车现在的混合动力系统全部为水冷式，而非空冷式。混合动力车在前格栅的发动机室内配置了不同于发动机用散热器的混合动力系统专用散热器。混合动力系统采用冷却水来冷却PCU和驱动马达。 图2：PCU（功率控制单元）主体由控制底板电路、双面散热的功率半导体元件、层叠型冷却器及电容器等构成。PCU内的功率半导体从两面进行冷却。过去采用的是单面冷却。 过去，丰田汽车的“普锐斯”及“皇冠Hybrid”等车型一直利用水冷单面冷却PCU内的功率半导体。 而“雷克萨斯LS600h”采用的最新PCU虽然同样是水冷式，但采用的是双面冷却构造（图1，2）。由于散热面积增大，因此比单面冷却更容易冷却。单位体积的输出功率比原来提高了60％。在相同的输出功率情况下，体积则可比原来减小约30％，重量减轻约20％。 PCU具有逆变器和升降压转换器的作用。逆变器具有将充电电池的直流电压转换成马达驱动用交流电压的功能以机将马达再生的交流电压转换成直流电压的功能。升降压转换器用来升高和降低充电电池供应给马达的电压。 向雷克萨斯LS600h等高功率混合动力车提供PCU，需要提高逆变器和升降压转换器的输出功率，也即需要增大电流。解决方法之一是增加PCU的功率半导体元件数量或使元件比原来流过更大电流。PCU存在问题是散热。现在的车载用功率半导体最高可耐150℃高温，因此需要采用始终将温度保持在150℃

以下的冷却结构。雷克萨斯LS600h需要提高PCU的性能，同时减小PCU尺寸。由于不能增加元件数量，因此采用了支持更大电流的功率半导体。 图3：过去的PCU构成（单面冷却）每个功率半导体元件流过200A，元件散热措施设想采用单面冷却时。 图4：新型PCU的构成（双面冷却）通过采用高性能功率半导体，每个元件流过300A以上的电流。采用支持大电流的元件，减少元件数量以实现小型化。通过双面冷却进行散热。( 这样，单面冷却就不足以解决大电流功率半导体的散热问题，因此采用了双面冷却结构。过去，每个元件可流过200A的电流，而雷克萨斯LS600h采用了每个元件可流过300A以上电流的高性能功率元件（图3、4）。由此逆变器和升降压转换器均减少了功率半导体的数量。新型功率半导体为富士电机元件科技制造的产品。（未完待续：特约撰稿人：金子高久，电装EHV机器技术部组长） 【电动汽车拆解】PCU（二）：实现了与铅蓄电池相当的尺寸 雷克萨斯LS600h是在高级轿车“雷克萨斯LS460”基础上追加混合动力系统而成。如果是混合动力专用车，PCU的尺寸或许会更大一些，而雷克萨斯LS600h 最优先强调的就是要减小PCU的尺寸。LS460将置于车辆前部的铅蓄电池移至车辆后部，PCU的尺寸只能与空出的铅蓄电池容积相当。

F6门禁管理系统用户手册

F6门禁管理系统用户手册 目录 1.系统软件 (2) 2.服务器连接 (2) 3.系统管理 (3) 3.1系统登录 (3) 3.2修改密码 (3) 4.联机通讯 (4) 4.1读取记录 (4) 4.2自动下载数据 (5) 4.3手动下载数据 (5) 4.4实时通讯 (6) 4.5主控设置 (6) 5.辅助管理 (8) 5.1服务器设置 (8) 5.2系统功能设置 (9) 5.3读写器设置 (10) 5.4电子地图 (13) 6.查询报表 (14) 6.1开锁查询 (14) 7.帮助 (18) 7.1帮助 (18)

1.系统软件 图1 门禁管理软件主界面 F6版门禁管理系统的软件界面如上图，顶端菜单栏包括“系统管理”、“联机通讯”、“辅助管理”、“查询报表”和“帮助”菜单；左侧快捷按钮包括“系统管理”、“联机通讯”、“辅助管理”、“查询报表”、“状态”等主功能项，每个主功能项包含几个子功能，在主界面上可以不依靠主菜单，就可在主界面中找到每个功能的快捷按钮。以下按照菜单栏的顺序进行介绍。 2.服务器连接 如图2点击设置则进入远程服务器设置，此处的远程服务器IP地址不是指数据库服务器，而是指中间层Fujica Server服务管理器的IP地址。 图2 服务连接

图2 远程服务器设置 3.系统管理 3.1系统登录 系统默认的操作员卡号为“0001”，密码为“admin”，上班人员输入管理卡号和密码后可以进入系统，进行授权给他的一切操作。 图3 系统登录 3.2修改密码 修改密码是指操作员登录成功后，可以修改自己登录的密码。先输入操作员的旧密码，再输入新密码并确认，则密码修改成功。

报废汽车回收拆解行业情况汇报

报废汽车回收拆解行业情况汇报为切实加强报废汽车回收拆解行业管理，规范交易行为，营造良好秩序，维护公共安全和社会稳定，提升报废汽车回收拆解行业安全生产管理水平。现将县报废汽车回收拆解行业现状汇报如下。 一、基本情况 为了加强报废汽车回收拆解行业规范管理，5月19日县商务局组成检查组，会同县公安局、县工商质监局和县环保局认真开展报废汽车回收拆解行业专项摸底、检查工作。主要检查企业的经营资格、证照资质持证情况和安全生产管理情况。 经过检查，目前，全县有两家报废汽车回收企业在进行报废汽车回收拆解业务，分别是市智发物资再生利用有限公司报废汽车回收站和市再生资源利用有限公司县分公司两家企业。市智发物资再生利用有限公司报废汽车回收站公司地址位于：县太和大道北段，该企业具备营业执照、省商务厅的批文和公安治安管理备案，xx年未办理环境影响评价资料；市再生资源利用有限公司县分公司地址位于：县沱牌镇五显楼村，该企业只有营业执照，没有其他相关证照。 二、处理情况 12345热线举报市再生资源利用有限公司县分公司，在没有商务厅的备案准入资质和环保手续的情况下擅自开展回收拆解报废汽车业务。通过县商务局调查了解后，分别于6月5日和6月25日给县车管所、县工商和质监管理局送去商函，要求停止对市再生资源利用有限公司县分公司的回收拆解报废汽车监消业务和违规经营行为。

在7月9日至7月13日期间连续4次接到12345热线举报市智发物资再生利用有限公司报废汽车回收站环境污染问题，反映该公司生产期间有烟雾、臭味和油污污染等现象。7月9日和7月16日县商务局会同县环保局执法大队的同志一道到城北智发报废汽车回收拆解站现场调查了解该企业的环保问题，证实：该企业回收的废旧轮胎统一码放在一起储存，没有焚烧轮胎等塑料制品的现象；在平时氧气切割时，保证先拆除可燃易燃物体后再进行氧割，在氧割期间不会产生很大的烟雾；在报废汽车拆解过程中产生的废柴油和废机油，企业全都自用了，没有用完的机油都是用油桶装放，没有油污泄漏现象，更没有油污横流街道影响居民出行的现象。该报废汽车站离居民小区距离甚远，厂区内的基本作业操作不会有上述影响。该企业在报废汽车处理流程中虽未产生环境影响现象，但我们和环保执法大队执法检查过程中发现该企业xx年未作环境影响评价资料，根据环政法函[xx]31号精神，责令该企业停止经营活动，依法依规做好环境影响评价。根据我们走访调查，这几起12345信访投诉属于行业间的恶性竞争采取的报复性举报，不是周边居民的举报。 三、整改规范 县商务局通过对报废汽车回收拆解行业调查处理后，要求企业停业整改，并对整改工作提出五个方面的明确要求：一是在我县设立合法的报废汽车回收拆解站点资格需得到省、市商务主管部门进行备案认定。二是进一步规范车辆收购、拆解行为，加强安全作业管理，确保拆解人员的安全。三是要落实整改，要严格按照技术规范和环保要

智能门禁管理系统说明书.doc

ID一体式/嵌入式门禁管理系统 使用说明书

1 软件使用说明 （1）配置要求 在安装软件之前，请先了解您所使用的管理电脑的配置情况。本软件要求安装在（基本配置）： Windows 2000，windows xp操作系统； 奔腾II600或更高的处理器(CPU)； 10GB以上硬盘； 128MB或更大的内存； 支持分辨率800*600或更高的显示器。 （2）安装说明 在光盘中运行“智能一卡通管理系统”安装程序（ID版），按照安装提示依次操作即可。 安装数据库以后，有两种创建数据库的方式，手动创建和自动创建。手动创建：在数据库SQL Server2000的数据库企业管理器中，建立一个database(数据库)。进入查询分析器/Query Analyzer 运行智能一卡通管理系统的脚本文件，形成门禁数据库表；自动创建：在安装智能一卡通管理软件中自动创建默认门禁数据库，默然数据名：znykt。 上述安装完后，在安装目录下,在first.dsn 文件中设置其参数，计算机server的名字（无服务器时即本机名）和数据库database的名字。 在桌面运行智能一卡通管理系统运行文件，选择卡号888888，密码为123456即可进入系统。 2 人事管理子系统 部门资料设置 首先运行‘智能一卡通管理系统’软件后，进入软件主界面，如下图所示：

然后点击进入“人事管理子系统”，如图所示： 选择<人事管理>菜单下的<部门管理>或点击工具栏内的‘部门管理’按钮，则会出现如下所示界面： 在<部门管理>中可以完成单位内部各个部门及其下属部门的设置。如果公司要成立新的部门，先用鼠标左键单击最上面的部门名，然后按鼠标右键弹出一菜单，在菜单中选择“增加部门”，则光标停留在窗口右边的“部门编号”输入框中，在此输入由用户自己定义的部门编号后，再在“部门名称”输入框中输入部门名称，最后按 <保存>按钮，此时发现窗口左边的结构图中多了一个新增的部门。如果要给部门设置其下属部门，则首选用鼠标左键选中该部门，再按鼠标右键弹出一菜单，在菜单中选择“增加”，最后输入、保存。同时也可以对选中的部门或下属部门进行“修改”或“删除”。特别要注意的是，如果是“删除”,则被选中的部门及其下属部门将被全部删除，所以要特别谨慎。

汽车拆装心得体会

汽车拆装心得体会 篇一：拆汽车心得体会 为期一周的汽车基础科学实验已经接近尾声了，两天的拆装发动机以及汽车底盘构件也算是对汽车有了一个系统的了解。 汽车拆装实习周用她缓慢的蹒跚似地脚步终于走过来了，我心情自然十分的激动，要知道作为一名车辆工程专业的学生，我觉得汽车构造非常的重要，是以后学习工作的基础，经过很长一段时间的理论学习之后，进行汽车拆装的实习可以加强我们对汽车构造的更深一步的了解，让很多的疑问得到解决，以及书上的一些抽象的知识具体化，让我们更深入的学习了这些知识。 第一天下午是动员大会，其实不用动员我们都已经很激动了。但是跟周老师熟悉熟悉也是好事，也便于明天的拆装工作能够顺利地进行。老师给人的第一印象就是，有激情。幸亏不是什么文质彬彬的理论哥来给我们知道，我们需要的是拥有大量实践经验的指导老师，而不是纸上谈兵的研究者。动员大会上了解到实习流程和规矩就回去准备明儿的实干了。 第二天，带着组员兴高采烈地奔往汽车大楼。来到了实习大楼的实习车间，进去后看到里面的发动机的时候，我的心中有种兴奋感，我很喜欢跟汽车打交道的，就像是跟一

个好朋友在一起的感觉似的。在老师的带领下熟悉了车间，然后老师讲解了流程和工具的操作和用途。这天我们进行了发动机的拆装。这次是在想好拆装的顺序，以及搞懂其工作原理之后进行的拆装，这样达到了事半功倍的效果，不仅速度快了，而且每一步都清楚的了解了其功用以及工作的原理。知道了配气机构的构成以及正时齿轮和正时皮带轮的安装，对曲柄连杆机构也有了具体的认识，清楚的认识了工作气缸的顺序，以及活塞连杆组的基本构成和安装顺序，点火系统的基本构成，以及工作原理，还有分电器的工作原理。因为之前的金工实习也有了解过发动机，但是没有拆过，所以激动的心情还是久久不能平静。 第二天是拆汽车底盘上的一些机构：变速器，转向器，制动器三个。变速器在金工实习时候拆过了，所以做起来比较熟手，而转向器和制动器的机构都很简单所以不到两小时就基本搞定了，就在看墙上的一些其他机构，像汽车的悬架，ABS系统等。还有旁边有一个电喷型的汽油发动机，比昨天拆的化油器式发动机是先进了点的东西，也进行了一番了解，也算不枉此行。但总的来说没有第一天的激动了。中午吃过饭在实验室休息了一下就回宿舍补觉了。 三个难忘片段： 一：拆发动机时的激动片段，全组人员都激动得差点不能自已。但是还是强行将自己激动的心情给压制下来了，

汽车电气拆装实习报告doc

汽车电气拆装实习报告 汽车电器拆装实习报告 实习内容： 一、传统点火系统的检测 点火系统有点火开关控制，点火开关有四个接线柱一般为B+、ACC、IG、STA。通过万用表对这四个接线柱进行判断，将万用表调至欧姆档通过表笔检测任意两个接线柱，常火线为主电源线B+，开关转动一档测量B+与剩下的线柱有显示的为ACC，依次则为IG、STA。然后将点火开关与传统点火系统相连接，接通电源观察点火放电现象。 二、电子点火系统 电子点火系统由分电器、点火线圈、点火模块等组成。分电器又分为磁电式和霍尔式，一般磁电式有两根接线柱均为信号线，霍尔式有三根接线柱为信号线、搭铁、正极线。将分电器、点火线圈、点火模块与电源相连，观察点火现象。点火模块通过信号线控制点火线圈点火。 三、微机点火系统 微机点火系统通过输出正极或负极信号控制点火。 四、起动机的测量与拆解检修汽车起动机的控制装置包括电磁开关、起动继电器和点火起动开关灯部件，其中电磁开关于起动机制作在一起。 、电磁开关 1.电磁开关结构特点电磁开关主要由电

磁铁机构和电动机开关两部分组成。电磁铁机构由固定铁心、活动铁心、吸引线圈和保持线圈等组成。固定铁心固定不动，活动铁心可以在铜套里做轴向移动。活动铁心前端固定有推杆，推杆前端安装有开关触盘，活动铁心后段用调节螺钉和连接销与拨叉连接。铜套外面安装有复位弹簧，作用是使活动铁心等可移动部件复位。电磁开关接线的端子的排列位置如图所示 2.电磁开关工作原理当吸引线圈和保持线圈通电产生的磁通方向相同时，其电磁吸力相互叠加，可以吸引活动铁心向前移动，直到推杆前端的触盘将电动开关触点接通势电动机主电路接通为止。当吸引线圈和保持线圈通电产生的磁痛方向相反时，其电磁吸力相互抵消， 在复位弹簧的作用下，活动铁心等可移动部件自动复位，触盘与触点断开，电动机主电路断开。 、起动继电器起动继电器的结构简图如图左上角部分所示，由电磁铁机构和触点总成组成。线圈分别与壳体上的点火开关端子和搭铁端子“E”连接，固定触点与起动机端子“S”连接，活动触点经触点臂和支架与电池端子“BAT”相连。起动继电器触电为常开触点，当线圈通电时，继电器铁心便产生电磁力，使其触点闭合，从而将继电器控制的吸引线圈和保持线圈电路接通。 、控制电路 1、控制电路包括起动继电器控制电路和起动机电磁开关控制电路。

博克门禁系统使用说明书

《门禁系统使用说明书》

陕西********科技有限公司 单位地址：**************************** 联系电话：**************************** 目录 （ 1.1）软件系统---------------------------------------------------------------------------------------1-135 第一章软件基本操作...................................................................................................................... - 5 - 2.1进入操作软件 (5) 2.4人事管理 (7) 2.4.1 企业信息.................................................................................................................................................................. - 7 - 2.4.2添加/编辑部门信息 ................................................................................................................................................ - 9 - 2.4.2.1添加部门 ............................................................................................................................................................... - 9 - 2.4.2.2修改部门 ............................................................................................................................................................ - 10 - 2.4.2.3 删除部门 ........................................................................................................................................................... - 11 -

废旧汽车拆解回收产业调研分析报告2

题目:废旧汽车拆解回收产业调研分析报告 学生姓名：郭盛 学院：机械与汽车工程学院 专业：车辆工程 班级1401 学号：1410340093 课程名称：废旧汽车拆解回收产业调研分析

一、废旧汽车拆解回收产业概述 废旧汽车是指汽车在达到一定使用年限或者车辆在一段时间的时候失去了使用价值或消费者认为它已经不能满足需求。这些废旧汽车如果不能得到很好的回大量的废旧汽车被随处丢弃、拼装车黑市流通、车辆中的某些物质对环境污染严重。而且汽车中富含大量的资源 金属、可重复利用材料等等不被很好的利用就会造成很大的资源浪费。所以废旧汽车拆解回收产业越来越受到各界的重视。废旧汽车的回收就是把这些资源重新利用起来 将有利用价值的材料和零部件从中分离出来 以新的产品或者经检验合格后重新投入市场 二、废旧汽车拆解回收产业主要特征 废旧汽车拆解回收的特征最主要表现在首先待回收汽车的分散性 具体是汽车回收产品的地点、时间和数量难以确定 因而回收运作的难度大 具有分散性和多对一的结构。其次表现在废旧汽车处理方法的不确定性 根据回收汽车损坏情况不同 需要对其进行不同处理。同时 回收汽车情况的不确定性造成产品加工时间的不确定和原材料需求的不确定。最后就是价值递增性 对于需要回收的汽车产品而言 它对消费者没有使用价值 但经过再处理 又重新获得其价值。 三、废旧汽车拆解回收产业发展的作用 1、经济效应 首先 提高资源的利用率 降低生产成本。汽车产业是一个

高耗能产业 能源、钢材的耗用很大 而且这些都是稀缺资源。在当今能源紧缺的情况下 汽车生产企业如何有效利用和配臵资源关系到企业的发展战略。充分发挥汽车回收产业的作用 能给企业带来巨大的效 益。 2、环境效应 随着社会环保运动的兴起、消费者环境意识的增强以及企业自身发展的需要和环境政策法规的制约 开展废旧汽车回收活动势在必行。不仅是企业自身实现可持续发展的重要推动力量 也是整个社会可持续发展的重要保证。通过对废旧汽车的有效回收管理 尽可能提高资源的利用率 减少对环境的破坏 由此产生良好的环境效应。 3、社会效益 废旧汽车回收是以实现资源使用的减量化、产品的反复使用和废弃物的资源化为目的 强调“清洁生产” 是一个“资源-产品-再生资源”的环状反馈式循环过程 最终实现“最优生产 最适消费少废弃”。是一种保护环境、降低资源消耗的可持续发展策 具有重要的社会价值。另外 汽车回收产业作为新兴的产业具有良好的发展前景 创造更多的就业机会 使社会生活稳定 有利于获得更多的政府支持和树立良好的企业形象。 四、我国废旧汽车拆解回收产业现状 在2010年7月国务院法制办发布《报废机动车回收拆解管

门禁系统使用说明书

-- - XX职业技术学院信息工程学院 门禁管理系统 操作说明书

制作人：X珍海 日期：2014年3月25日 目录 (请打开【帮助H】下的【使用说明书】，这样方便您了解本系统) 第1章软件的基本操作3 1.1 登录和进入操作软件3 1.2 设备参数设置4 1.3 部门和注册卡用户操作4 1.3.1 设置部门4 1.3.2 自动添加注册卡功能（自动发卡）5 1.4 基本操作7 1.4.1 权限管理8 1.4.2 校准系统时间11 1.5 常用工具12 1.5.1 修改登陆用户名和密码12 第2章考勤管理功能模块13 2.1 正常班考勤设置13 2.1.1 设置考勤基本规则13 2.1.2 设置节假日和周休日14 2.1.3 请假出差的设置15 2.2 考勤统计和生成报表17 2.2.1 生成考勤详细报表17 2.2.2 启用远程开门错误!未定义书签。

第1章软件的基本操作 1.1登录和进入操作软件 1．点击【开始】>【程序】>【专业智能门禁管理系统】>【专业智能门禁管理系统】或双击桌面钥匙图标的快捷方式，进入登录界面。 2．输入缺省的用户名：abc 与密码：123（注意：用户名用小写）。该用户名和密码可在软件里更改。 3．登录后显示主操作界面

入门指南。如果您没有经验，您可以在该向导的指引下完成基本的操作和设置。我们建议您熟悉后, 关闭操作入门指南，仔细阅读说明书，熟悉和掌握软件的操作。 “关闭入门指南”后，操作界面如下。 1.2设备参数设置 1.3部门和注册卡用户操作 1.3.1设置部门 点击【设置】>【部门】，进入部门界面。 点击【添加最高级部门】。

2017年报废汽车拆解行业分析报告

2017年报废汽车拆解行业分析报告 2017年1月

目录 一、行业发展概况 (4) 1、我国报废汽车拆解行业发展概况 (4) 2、国外报废汽车拆解行业发展概况 (7) 二、行业市场空间 (10) 1、汽车拆解行业潜力无限，未来市场发展空间巨大 (10) 2、汽车拆解行业在环保行业中的地位提升，得到政府的高度重视 (11) 3、黄标车整治将成为汽车拆解行业的催化剂 (11) 三、行业发展趋势 (13) 1、今后的十年汽车报废将呈持续增长趋势 (14) 2、报废汽车回收拆解企业全部实施升级改造 (14) 3、报废汽车回收拆解行业结构优化，有条件的建立区域性破碎示范中心 .. 15 4、汽车零部件再制造业务，将和报废汽车回收拆解行业更紧密的结合 (15) 5、加快建立起功能齐全的网络服务平台 (15) 四、行业监管体系和产业政策 (16) 16 1、行业监管体系 .................................................................................................. 17 2、行业相关法律法规规章 .................................................................................. 22 3、质量标准 .......................................................................................................... 五、进入行业的主要障碍 (22) 22 1、行政许可证资格 .............................................................................................. 22 2、环保规模 .......................................................................................................... 23 3、技术人才 ..........................................................................................................

2017年汽车拆解行业分析报告

(此文档为word格式，可任意修改编辑！）

正文目录 一、国内汽车拆解市场基础逐步夯实，汽车保有量仍将持续增长 . 4 1．近年国内汽车行业继续呈现高速发展势头，年产销量屡创新高 4 2．我国千人汽车保有量仍远低于发达国家，汽车存量发展空间大 5 二、报废汽车回收拆解行业：未来2-3年有望进入较快发展阶段 . 6 1．汽车拆解：通过可用零部件、废金属获得回收受益 (6) 2．我国报废汽车回收拆解业有望进入新的发展阶段 (7) 3．目前我国报废汽车回收拆解行业稳步发展 (9) 4．政策松绑助推行业发展 (11) 四、汽车拆解市场空间广阔，未来有望逐步达千亿元 (12) 1．中短期的市场依靠黄标车和老旧车的淘汰 (13) 2．长期市场依靠存量车的淘汰和正规回收率的提高 (15) 五、主要公司分析 (16) 六、风险提示 (18)

图表目录 图表1：2016年国内汽车产销量均突破2800万辆 (4) 图表2：2017Q1，全国汽车保有量突破2亿辆 (5) 图表3：我国千人汽车保有量低于世界平均水平，远低于发达国家 (6) 图表4：汽车注销、报废、拆解的流转过程 (7) 图表5：国内报废汽车回收拆解行业发展稳步推进 (9) 图表6：2014年起开始报废汽车回收量明显增加 (10) 图表7：近年国内的汽车回收量稳中有升，实际回收率依旧偏低11 图表8：近年我国关于汽车拆解出台的系列政策 (12) 图表9：正规渠道回收车辆占比只有近一半 (13) 图表10：车辆拆解产值中钢铁占比最大，7成左右 (13) 图表11：中国黄标车数量2013年约有1300万辆 (15) 图表12：中国汽车注销比例远低于发达国家 (15) 图表13：预计2020年汽车回收行业产值将约千亿元 (16) 图表14：国内报废汽车回收拆解行业的相关上市公司 (18)

废旧汽车拆解回收及加工建设项目可行性研究报告

废旧汽车拆解处理项目可行性报告 废旧汽车拆解回收及加工项目可行性研究报告 ############零点企业管理咨询中心 二零一一年十二月

目录 第一章总论··············错误！未定义书签。 1.1项目概况··················错误！未定义书签。 1.2建设单位概况················错误！未定义书签。 1.3建设内容及规模···············错误！未定义书签。 1.4投资估算及资金筹措·············错误！未定义书签。 1.5报告编制依据················错误！未定义书签。 1.6项目实施周期················错误！未定义书签。 1.7主要经济技术指标表·············错误！未定义书签。 1.8编制原则及指导思想·············错误！未定义书签。 1.9结论····················错误！未定义书签。第二章产业政策及项目建设必要性····错误！未定义书签。 2.1我国面粉加工业产业政策···········错误！未定义书签。 2.2我国面粉行业的现状·············错误！未定义书签。 2.3当地面粉行业现状··············错误！未定义书签。 2.4项目建设的必要性··············错误！未定义书签。第三章市场分析与营销方案······错误！未定义书签。 3.1市场分析··················错误！未定义书签。 3.2项目产品的市场竞争优势分析·········错误！未定义书签。

第四章项目建设条件··········错误！未定义书签。 4.1厂址选择原则················错误！未定义书签。 4.2项目厂址··················错误！未定义书签。 4.3建设条件··················错误！未定义书签。第五章技术方案、设备方案和建设方案··错误！未定义书签。 5.1建设规划和布局原则·············错误！未定义书签。 5.2工艺技术方案················错误！未定义书签。 5.3主要设备方案················错误！未定义书签。 5.4总平面布置·················错误！未定义书签。 5.5工程建设方案················错误！未定义书签。 5.6配套工程··················错误！未定义书签。第六章环境影响分析··········错误！未定义书签。 6.1编制依据··················错误！未定义书签。 6.2施工期污染源及污染物············错误！未定义书签。 6.3施工期的环境保护对策············错误！未定义书签。 6.4运营期污染源及污染物············错误！未定义书签。 6.5项目运营期污染物治理············错误！未定义书签。第七章节能措施············错误！未定义书签。

门禁系统管理平台-详细设计说明书

门禁系统管理平台详细设计报告 2015年09月20日

目录 一、基本信息 .................................................................................................................. 错误！未定义书签。 二、市场分析 (4) 1．客户需求分析 (4) （1）国际国内市场需求量预测及客户咨询类似产品情况..... 错误！未定义书签。 （2）客户对该产品的功能、安全、使用环境要求等............. 错误！未定义书签。 2．市场现状分析 (4) 三、详细设计 (4) 1. 模块描述 (4) 2. 功能描述 (4) 3. 信息传输过程 (6) 4. 标准符合性分析 (6) 5. 验证（试制/试验/检测）确认方法、手段的分析 (8) 四、资源论证 (8) 1．人力资源需求分析 (8) 2．开发设备资源需求分析 (9) 3．项目开发成本预算 (9) 五、研发时间安排 (9) 六、项目风险评估 (10) 1．技术方面 (10) 2．人员方面 (10) 3．其它资源 (10) 七、评审结论 (11) 八、公司意见 (11)

一、市场分析 1．客户需求分析 1.2014年7月份由三大运营商出资成立了中国通信设施服务股份有限公司，同年9月份 变更名称为中国铁塔股份有限公司。铁塔公司成立后，2015年12月下旬，2000多亿存量铁塔资产基本完成交接。而从2015年1月1日起，三大运营商停止新建铁塔基站，交由中国铁塔进行建设。据统计，2015年1-11月，中国铁塔累计承接三家电信运营企业塔类建设需求53.2万座，已交付41.8万座。针对如此庞大的存量基站及新建基站。 铁塔公司总部急需对基站人员进出做到统一管理，有效管控。提高效率。因此所产生的市场需求量是很大的。 2.随着互联网及物联网技术的快速发展，原有传统门禁管理系统、单一功能的管理软件已 经无法管理众多不同品牌、不同通讯方式、不同厂家的IC/ID读卡设备，因此客户需要一种开放式、分布式的云管理平台，来管理整个基站门禁系统中的所有设备 2．市场现状分析 ●同行业中，各厂家的产品采用传统的门禁方案，既读卡器和控制器及电磁锁或电插锁对 现场的基站门进行管理。造价昂贵，安装复杂。。 ●目前大部分厂家的管理平台架构单一，系统兼容性差，各家的门禁管理平台只能兼容自 家的控制器。开放性不够。 ●目前很多厂商的平台都是针对某一个硬件厂商的设备来运行的，当项目中有多家设备时 平台的控制力明显不足 二、详细设计 1. 模块描述 铁塔基站门禁系统管理平台系统主要包括三部分：BS/CS客户端、云服务器和手机APP。 其中客户端的主要功能包括： 支持对多家基站锁具设备的识别、获取、登录 支持对不同用户进行权限划分。 支持对锁具根据区域进行分组。 支持多家基站锁具设备的设备配置 支持多家设备通过手机APP开锁、获取状态、日志查询。 支持多家设备的设备时间校准 支持设备更新，当设备更新时，可以方便的只更新涉及到的文件，而不需要重装整个系统 支持电子地图

汽车发动机拆装分析报告

汽车发动机拆装报告

————————————————————————————————作者：————————————————————————————————日期： 2

汽车发动机拆装 实训报告 班级：汽电1501 姓名：缪维广 学号：201530051 西南科技大学城市学院机电工程系 2016年4月

AJR发动机拆装实训报告 一、实训项目 (一)对桑塔纳2000发动机进行拆卸，安装 (二)对气缸体平面度的检测 （三）气缸磨损检测 二、实训目的 （一）掌握AJR发动机的结构组成与工作原理 （二）发动机主要部件的装配关系与运动情况 （三）掌握发动机的拆装流程 （四）工具量具和仪器的名称及使用。 三、实训器材 （一）桑塔纳2000GSI型轿车 （二）拆装翻架和可正常运行的发动机 （三）汽车维修常用工具和大众专用拆装工具：桑塔纳2000上的AJR发动机、工具箱、零件摆放桌。大号、中号荆轮扳手，11mm.10mm六角公制套筒，接杆，中号万向接头，大转中接头，扳手，扭力扳手，活塞环压缩器，扳手，中孔花型旋具头。内六角扳手。金属刷子或刮刀，刀口型直尺，塞尺，游标卡尺，千分尺，百分表，量缸表。 （四）存放零部件工作台 四、实训时间及地点 （一）时间：2016年3月—4月周二上午及周四下午

(二)地点：二教107 五、小组成员与分配情况 （一）小组成员：赵艺杨、李奕谷、尹航宇、彭启瑞、缪维广、黄鑫 （二）分配情况：黄鑫主要拆装发动机支架，进气歧管，排气歧管，正时同步带。缪维广主要拆卸气缸部分。彭启瑞和李亦谷主要拆卸油底壳，机油泵，挡油板发动机活塞连杆机构。赵艺杨负责工具的寻找，提醒工作顺序。尹航宇负责记录在拆卸过程中零部件的损失情况，查漏补缺，装配时谁拆谁装配。 六、实训内容 （一）AJR发动机的拆解过程 1.拔下机油尺 2.拆卸进气（排气、水泵支架、发动机支架）： （1）先用扳手扭松进气（排气、水泵支架、发动机支架）歧管紧固螺栓（从两端向中间松） （2）再用快速扳手拆卸进气（排气、水泵支架、发动机支架）歧管紧固螺栓、螺母 （3）取下进气（排气、水泵支架、发动机支架）歧管（将衬垫、螺栓、进气歧管放在一起，避免与其他的螺栓混淆） 3.松开卡扣，取下正时同步带上防护罩 4.拆卸皮带盘 （1）预松曲轴皮带盘紧固螺栓（对角线松） （2）拆卸下曲轴皮带盘紧固螺栓 （3）取下曲轴皮带盘 5.拆卸中间防护罩

智能门禁管理系统说明书

IC一体式/嵌入式门禁管理系统 使用说明书

目录 1．系统简介 (3) 2．功能特点 (3) 3、主要技术参数 (4) 4、系统组成 (4) 5、设备连接 (5) 6、门禁管理系统软件 (6) 6.1 软件的安装 (6) 6.2 人事管理子系统 (7) 6.3 一卡通管理系统 (9) 6.4 门禁管理子系统 (12) 7. 调试操作流程 (28) 8、注意事项 (28)

1．系统简介 在高科技发展的今天，以铁锁和钥匙为代表的传统房门管理方式已经不能满足要求，而集信息管理、计算机控制、Mifare 1 IC智能(射频)卡技术于一体的智能门禁管理系统引领我们走进新的科技生活。 Mifare 1 IC智能(射频)卡上具有先进的数据通信加密并双向验证密码系统，卡片制造时具有唯一的卡片系列号，保证每张卡片都不相同。每个扇区可有多种密码管理方式。卡片上的数据读写可超过10万次以上；数据保存期可达10年以上，且卡片抗静电保护能力达2KV以上。具有良好的安全性，保密性，耐用性。 IC卡嵌入式门禁管理系统以IC卡作为信息载体，利用控制系统对IC卡中的信息作出判断，并给电磁门锁发送控制信号以控制房门的开启。同时将读卡时间和所使用的IC卡的卡号等信息记录、存储在相应的数据库中，方便管理人员随时查询进出记录，为房门的安全管理工作提供了强有力的保证。 IC卡嵌入式门禁管理系统在发行IC卡的过程中对不同人员的进出权限进行限制，在使用卡开门时门禁控制机记录读卡信息，在管理计算机中具有查询、统计和输出报表功能，既方便授权人员的自由出入和管理，又杜绝了外来人员的随意进出，提高了安全防范能力。 IC卡嵌入式门禁管理系统，在线监控IC卡开门信息、门状态，给客户以直观的门锁管理信息。 IC卡嵌入式门禁（简称门禁读卡器，门禁控制机，控制器）是目前同行业产品中体积较小的门禁，可以嵌入到市场上几乎所有的楼宇门禁控制器中，解决了因为楼宇门禁控制器内部空间小所带来的麻烦，是楼宇门禁控制器的最佳配套产品；它绝不仅仅是简单的门锁工具，而是一种快捷方便、安全可靠、一劳永逸的多功能、高效率、高档次的管理系统。它能够让你实实在在享受高科技带来的诸多实惠和方便。 2．功能特点 2．1．IC卡嵌入式门禁具有的功能： 2.1.1使用MIFARE 1 IC卡代替钥匙，开门快捷，安全方便。 2.1.2经过授权，一张IC卡可以开启多个门（255个以内）。 2.1.3可以随时更改、取消有关人员的开门权限。 2.1.4读卡过程多重确认，密钥算法，IC卡不可复制，安全可靠。 2.1.5具有512条黑名单。

报废汽车拆解再生利用项目可行性研究报告

第一章总论 第一节项目背景 一、项目名称及承办单位 项目名称：报废汽车拆解再生利用项目 承办单位：江苏博华环保科技有限公司 建设地点：响水县陈家港沿海经济区 建设性质：新建 企业类型：有限责任公司 隶属行业：废弃资源和废旧材料回收加工业 法定代表人：李霏 项目负责人：李霏 二、承办单位情况 江苏博华环保科技有限公司成立于2015年12月15日，是由自然人李霏、王兆娣等人共同投资组建的环保科技有限公司，拟建设30万辆/年报废汽车拆解再生利用生产线。项目选址于响水县陈家港沿海经济区，注册资本金2000万元，计划总投资7.2亿元，占地面积401亩。企业经营范围：废弃资料和废旧材料的回收、加工、销售；环境污染处理剂生产、销售；再生物质回收、销售；废弃资源循环利用技术的研究、信息咨询服务；水污染治理；固体废物治理；节能环保领域设备、技术的推广、咨询、转让、服务。 三、研究工作依据 1、《中华人民共和国土地管理法》； 2、《中华人民共和国土地管理法实施细则》； 3、《国务院关于投资体制改革的决定》，国发[2004]20号； 4、《产业结构调整指导目录(2011年本)》（2013年修正版）；

5、《江苏省工业和信息产业结构调整指导目录（2012年本）》；苏政办发〔2013〕9号文； 6、《江苏省企业投资项目备案暂行办法》；苏政发[2005]38号； 7、《江苏省建设用地指标体系》（2010年版）； 8、《投资项目可行性研究指南》； 9、《建设项目经济评价方法与参数》(第三版)； 10、《建设项目经济评价方法与参数及使用手册》（第三版）； 11、《中华人民共和国国民经济和社会发展第十三个五年规划纲要（十三五规划）》； 12、《中华人民共和国固体废物污染环境防治法（2015年修正）》； 13、《中华人民共和国节约能源法》； 14、《中华人民共和国可再生能源法》； 15、《中华人民共和国清洁生产促进法》； 16、《国家中长期科学和技术发展规划纲要（2006-2020）》； 17、《现代财务会计》； 18、《工业投资项目评价与决策》； 19、国家公布的相关设备及施工标准； 20、项目咨询合同书及企业提供的其它相关资料。 四、编制原则 1、坚持技术、设备的先进性、适用性、合理性、经济性原则，采用国内最先进的信息系统技术，确保产品质量，以达到企业的高效益。 2、认真贯彻执行国家基本建设的各项方针、政策和有关规定，执行国家及各部委颁发的现行标准和规范。 3、设计中尽一切努力节能降耗，节约用水，提高能源的重复利用率。 4、设计中注重环境保护及节能降耗，在建设过程中采用行之有效的环境综合治理措施。 5、注重劳动安全和卫生，设计文件应符合国家有关劳动安全、劳动卫生及消防等标准和规范要求。